We report on the discovery of a new fast radio burst (FRB), FRB 150215, with the Parkes radio telescope on 2015 February 15. The burst was detected in real time with a dispersion measure (DM) of 1105.6 +/- 0.8 pc cm(-3), a pulse duration of 2.8(-0.5)(+1.2) ms, and a measured peak flux density assuming that the burst was at beam centre of 0.7(-0.1)(+0.2) Jy. The FRB originated at a Galactic longitude and latitude of 24.66 degrees, 5.28 degrees and 25 degrees away from the Galactic Center. The burst was found to be 43 +/- 5 per cent linearly polarized with a rotation measure (RM) in the range -9 < RM < 12 rad m(-2) (95 per cent confidence level), consistent with zero. The burst was followed up with 11 telescopes to search for radio, optical, X-ray, gamma-ray and neutrino emission. Neither transient nor variable emission was found to be associated with the burst and no repeat pulses have been observed in 17.25 h of observing. The sightline to the burst is close to the Galactic plane and the observed physical properties of FRB 150215 demonstrate the existence of sight lines of anomalously low RM for a given electron column density. The Galactic RM foreground may approach a null value due to magnetic field reversals along the line of sight, a decreased total electron column density from the Milky Way, or some combination of these effects. A lower Galactic DM contribution might explain why this burst was detectable whereas previous searches at low latitude have had lower detection rates than those out of the plane.
A polarized fast radio burst at low Galactic latitude / Petroff, E; Burke-Spolaor, S; Keane, Ef; Mclaughlin, Ma; Miller, R; Andreoni, I; Bailes, M; Barr, Ed; Bernard, Sr; Bhandari, S; Bhat, Ndr; Burgay, M; Caleb, M; Champion, D; Chandra, P; Cooke, J; Dhillon, Vs; Farnes, Js; Hardy, Lk; Jaroenjittichai, P; Johnston, S; Kasliwal, M; Kramer, M; Littlefair, Sp; Macquart, Jp; Mickaliger, M; Possenti, A; Pritchard, T; Ravi, V; Rest, A; Rowlinson, A; Sawangwit, U; Stappers, B; Sullivan, M; Tiburzi, C; van Straten, W; Albert, A; Andre, M; Anghinolfi, M; Anton, G; Ardid, M; Aubert, Jj; Avgitas, T; Baret, B; Barrios-Marti, J; Basa, S; Bertin, V; Biagi, S; Borrnuth, R; Bourret, S; Bouwhuis, Mc; Bruijn, R; Brunner, J; Busto, J; Capone, A; Caramete, L; Carr, J; Celli, S; Chiarusi, T; Circella, M; Coelho, Jab; Coleiro, A; Coniglione, R; Costantini, H; Coyle, P; Creusot, A; Deschamps, A; De Bonis, G; Distefano, C; Di Palma, I; Donzaud, C; Dornic, D; Drouhin, D; Eberl, T; El Bojaddaini, I; Elsasser, D; Enzenhofer, A; Felis, I; Fusco, La; Galata, S; Gay, P; Geisselsoder, S; Geyer, K; Giordano, V; Gleixner, A; Glotin, H; Gregoire, T; Gracia-Ruiz, R; Graf, K; Hallmann, S; van Haren, H; Heijboer, Aj; Hello, Y; Hernandez-Rey, Jj; Hossl, J; Hofestadt, J; Hugon, C; Illuminati, G; James, Cwcw; de Jong, M; Jongen, M; Kadler, M; Kalekin, O; Katz, U; Kiessling, D; Kouchner, A; Kreter, M; Kreykenbohm, I; Kulikovskiy, V; Lachaud, C; Lahmann, R; Lefevre, D; Leonora, E; Lotze, M; Loucatos, S; Marcelin, M; Margiotta, A; Marinelli, A; Martinez-Mora, Ja; Mathieu, A; Mele, R; Melis, K; Michael, T; Migliozzi, P; Moussa, A; Mueller, C; Nezri, E; Pavalas, Ge; Pellegrino, C; Perrina, C; Piattelli, P; Popa, V; Pradier, T; Quinn, L; Racca, C; Riccobene, G; Roensch, K; Sanchez-Losa, A; Saldana, M; Salvadori, I; Samtleben, Dfe; Sanguineti, M; Sapienza, P; Schnabel, J; Seitz, T; Sieger, C; Spurio, M; Stolarczyk, T; Taiuti, M; Tayalati, Y; Trovato, A; Tselengidou, M; Turpin, D; Tonnis, C; Vallage, B; Vallee, C; Van Elewyck, V; Vivolo, D; Vizzoca, A; Wagner, S; Wilms, J; Zornoza, Jd; Zuniga, J; Abdalla, H; Abramowski, A; Aharonian, F; Benkhali, Fa; Akhperjanian, Ag; Andersson, T; Anguner, Eo; Arrieta, M; Aubert, P; Backes, M; Balzer, A; Barnard, M; Becherini, Y; Tjus, Jb; Berge, D; Bernhard, S; Bernlohr, K; Blackwell, R; Bottcher, M; Boisson, C; Bolmont, J; Bordas, P; Bregeon, J; Brun, F; Brun, P; Bryan, M; Bulik, T; Capasso, M; Casanova, S; Cerruti, M; Chakraborty, N; Chalme-Calvet, R; Chaves, Rcg; Chen, A; Chevalier, J; Chretien, M; Colafrancesco, S; Cologna, G; Condon, B; Conrad, J; Cui, Y; Davids, Id; Decock, J; Degrange, B; Deil, C; Devin, J; de Wilt, P; Dirson, L; Djannati-Atai, A; Domainko, W; Donath, A; Drury, Lo; Dubus, G; Dutson, K; Dyks, J; Edwards, T; Egberts, K; Eger, P; Ernenwein, Jp; Eschbach, S; Farnier, C; Fegan, S; Fernandes, Mv; Fiasson, A; Fontaine, G; Forster, A; Funk, S; Fussling, M; Gabici, S; Gajdus, M; Gallant, Ya; Garrigoux, T; Giavitto, G; Giebels, B; Glicenstein, Jf; Gottschall, D; Goya, A; Grondin, Mh; Hadasch, D; Hahn, J; Haupt, M; Hawkes, J; Heinzelmann, G; Henri, G; Hermann, G; Hervet, O; Hinton, Ja; Hofmann, W; Hoischen, C; Holler, M; Horns, D; Ivascenko, A; Jacholkowska, A; Jamrozy, M; Janiak, M; Jankowsky, D; Jankowsky, F; Jingo, M; Jogler, T; Jouvin, L; Jung-Richardt, I; Kastendieck, Ma; Katarzynski, K; Kerszberg, D; Khelifi, B; Kieffer, M; King, J; Klepser, S; Klochkov, D; Kluzniak, W; Kolitzus, D; Komin, N; Kosack, K; Krakau, S; Kraus, M; Krayzel, F; Kruger, Pp; Laffon, H; Lamanna, G; Lau, J; Lees, Jp; Lefaucheur, J; Lefranc, V; Lemiere, A; Lemoine-Goumard, M; Lenain, Jp; Leser, E; Lohse, T; Lorentz, M; Liu, R; Lopez-Coto, R; Lypova, I; Marandon, V; Marcowith, A; Mariaud, C; Marx, R; Maurin, G; Maxted, N; Mayer, M; Meintjes, Pj; Meyer, M; Mitchell, Amw; Moderski, R; Mohamed, M; Mohrmann, L; Mora, K; Moulin, E; Murach, T; de Naurois, M; Niederwanger, F; Niemiec, J; Oakes, L; O'Brien, P; Odaka, H; Ottl, S; Ohm, S; Ostrowski, M; Oya, I; Padovani, M; Panter, M; Parsons, Rd; Pekeur, Nw; Pelletier, G; Perennes, C; Petrucci, Po; Peyaud, B; Piel, Q; Pita, S; Poon, H; Prokhorov, D; Prokoph, H; Puhlhofer, G; Punch, M; Quirrenbach, A; Raab, S; Reimer, A; Reimer, O; Renaud, M; de los Reyes, R; Rieger, F; Romoli, C; Rosier-Lees, S; Rowell, G; Rudak, B; Rulten, Cb; Sahakian, V; Salek, D; Sanchez, Da; Santangelo, A; Sasaki, M; Schlickeiser, R; Schulz, A; Schussler, F; Schwanke, U; Schwemmer, S; Settimo, M; Seyffert, As; Shafi, N; Shilon, I; Simoni, R; Sol, H; Spanier, F; Spengler, G; Spies, F; Stawarz, L; Steenkamp, R; Stegmann, C; Stinzing, F; Stycz, K; Sushch, I; Tavernet, Jp; Tavernier, T; Taylor, Am; Terrier, R; Tibaldo, L; Tiziani, D; Tluczykont, M; Trichard, C; Tuffs, R; Uchiyama, Y; van der Walt, Dj; van Eldik, C; van Rensburg, C; van Soelen, B; Vasileiadis, G; Veh, J; Venter, C; Viana, A; Vincent, P; Vink, J; Voisin, F; Volk, Hj; Vuillaume, T; Wadiasingh, Z; Wagner, Sj; Wagner, P; Wagner, Rm; White, R; Wierzcholska, A; Willmann, P; Wornlein, A; Wouters, D; Yang, R; Zabalza, V; Zaborov, D; Zacharias, M; Zanin, R; Zdziarski, Aa; Zech, A; Zefi, F; Ziegler, A; Zywucka, N. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 469:4(2017), pp. 4465-4482. [10.1093/mnras/stx1098]
A polarized fast radio burst at low Galactic latitude
Trovato A;
2017-01-01
Abstract
We report on the discovery of a new fast radio burst (FRB), FRB 150215, with the Parkes radio telescope on 2015 February 15. The burst was detected in real time with a dispersion measure (DM) of 1105.6 +/- 0.8 pc cm(-3), a pulse duration of 2.8(-0.5)(+1.2) ms, and a measured peak flux density assuming that the burst was at beam centre of 0.7(-0.1)(+0.2) Jy. The FRB originated at a Galactic longitude and latitude of 24.66 degrees, 5.28 degrees and 25 degrees away from the Galactic Center. The burst was found to be 43 +/- 5 per cent linearly polarized with a rotation measure (RM) in the range -9 < RM < 12 rad m(-2) (95 per cent confidence level), consistent with zero. The burst was followed up with 11 telescopes to search for radio, optical, X-ray, gamma-ray and neutrino emission. Neither transient nor variable emission was found to be associated with the burst and no repeat pulses have been observed in 17.25 h of observing. The sightline to the burst is close to the Galactic plane and the observed physical properties of FRB 150215 demonstrate the existence of sight lines of anomalously low RM for a given electron column density. The Galactic RM foreground may approach a null value due to magnetic field reversals along the line of sight, a decreased total electron column density from the Milky Way, or some combination of these effects. A lower Galactic DM contribution might explain why this burst was detectable whereas previous searches at low latitude have had lower detection rates than those out of the plane.Pubblicazioni consigliate
I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
